# CONFIGURATION FILE TO EXECUTE GOODMAN ITC
# ==========================================

objname = 'UM 483'           # Name of the source
ra    = '12:38:50.94'          # Right ascension
dec   = '-49:47:58.8'          # Declination
epoch = '2000'                 # Equinox of the date
extragal = 'n'                 # Extragalactic source? [y/n]
distt = 5.0                    # Distance of the source [kpc]

# Mark with a "x" the nature of the source/spectrum which will be observed.
# Spectrum superpostion in not allowed at the moment, so choose only one
# category and erase the other.

spiral=''                      # Spiral galaxy
elliptical=''                  # Eliptical galaxy
hiireg=''                      # HII region
pn=''                          # Planetary Nebulae
qso=''                         # Quasar
star='x'                       # Star (LTT3218)

# Considerations about the photometry and geometry of the source

extended = 'n'                 # Is the source extended
mag=25                       # Integrated magnitude [mag] or surface bright-
                               # ness if the source is extended [mag/arcsec^2]
obsfilter='V'                  # Filter used for the magnitude above ['g', 'r', 
                               # 'B', I, R, U, V]
seeing=0.9                     # Image quality [arcsec]
razax=0.0                      # Ellipticity of the source
size=0.0                       # Source sky size [arcsec]
PA=0                          # PA of the major axis [degrees]

# The radial movement of the source

velrad = 0.0                   # Radial velocity [km/s]
redshift = ''                  # Redshift (if more convenient than tha velrad)

# Spectral region to be observed

lambda0 = 4861                 # Central wavelength [Angstroms]
resolution = 2800              # Spectral resolution
fracdlambda = 0.8              # Fraction of the free spectral range
                               # to be effectively observed. It can
                               # reduce the observation time if only a part
                               # of the spectral range is interesting for
                               # your purposes.

# OBSERVATION SITE
# ================

# General information about the SOAR site

soarlong=-70.733722            # Site longitude [Degrees]
soarlati=-30.238000            # Site latitude  [Degrees]
soaralti=2738.0                # Site altitude [meters]
soartemp=6.84                  # Mean temperature at SOAR
soarpres=724.76                # pressure (mBar) at the SOAR Telescope elevation,
                               # using the International Standard Atmosphere


# OBSERVATION MODE AND DETAILS ABOUT IT
# =====================================

# Information concerning the two possible observation modes at SOAR: the
# classical, for which the obervation is previously known and the queue mode
# in which only the maximum airmass can be controled by the observer.

queueclassic='queue'           # Observation mode. Attention to this because if
                               # you are going to observe in classical mode the
                               # results can be optimized. Otherwise the worst
                               # condictions at the limite of the observer's
                               # tolerance will be considered

date='2009/7/8'                # In case of a classic observation, date of the
                               # observation [Universal Time]

hour='02:43:17'                # In case of a classic observation, hour of the
                               # observation [Universal Time]

acceptableairmass = 1.24        # Maximum acceptable airmass
                               

# CONFIGURATION OF THE GALACTIC EXTINCTION
# ========================================

# Parameter to run the EXTIN procedure by Amores & Lepine (2005)
# conveted to python by Sergio Scarano Jr jun 2009.

r0=7.5                         # adopted distance of the Galactic center
stepp=0.05                      # steps of the gas density integration to
                               # obtain column density, in pc

                                
# General parameters to introduce the galactic extinction in the observed
# spectrum.

R_V = 3.1


# MAXIMUM ACCEPTABLE SKY BACKGROUND
# ==================================

# Paramenters used to calculate the sky noise in the queue mode. It reflect
# the maximum acceptable sky brightness, related to the fraction of the
# which is illuminated.

skyback='20%'    # Choose: 20%, for the worst level in the darkest range 
                 #         50%, for the worst level in the dark range
                 #         80%, for the worst level in the gray range
                 #         any, for the worst level at all

# Cloud Cover
# ============

# Fraction of the light lost through the clouds.

cloucov=0.


   # Choose: 20%, for the worst level in the darkest range 
                 #         50%, for the worst level in the dark range
                 #         80%, for the worst level in the gray range
                 #         any, for the worst level at all                 

# VARIABLES RELATED TO THE TELESCOPE
# ==================================

# Details about the telescope.

teldiameter = 4.1                      # diameter of the telescope in meters


# VARIABLES RELATED TO THE INSTRUMENT
# ===================================

# Information about the grating and observation mode.

grating='300'                          # grating and observation mode. the
                                       # possible values are 300, 600b,
                                       # 600r(GG-495), 1200m1, 1200m3, 1200m5
                                       # and 1200m7

# Slit size

slit='3.00'                            # the options are: 0.46, 0.84, 1.03
                                       # 1.35, 3.00, 10.0, Big slit.

# Information about the CCD.

rr = '100'           # pixel readrate in kHz. possible values 400, 200, 100, 50
att = '3'            # attenuation index
npixels = 512**2     # total amount of pixels in the CCD
pixsize=0.15         # Pixel size [arcsec/pix]
binning=2            # binning: use 1 for 1x1, 2 for 2x2 and 4 for 4x4.
bin_x=1
bin_y=1


# DETAILS TO CALCULATE THE EXPOSTION TIME INTEGRATION
# ===================================================

# Setting the way the integration time calculations will be performed.


snrintgr='r'        # set this parameter to 's' if you want calculate how much
                    # time you need to get a certain value of snr to the most
                    # proemint feature in the spectrum.

sndesire=25      # the minimum signal-to-noise ratio desired.

limittime=1000.0   # limit time in seconds. It must be improved to automatically
                    # receive the amount of time the source will be above the
                    # horizon inside the period of time for the astronomical
                    # sunrise and sunset.

exptime=300       # integration time in seconds to be used in case of
                    # snrintgr='n'. It will provide the signal-to-noise ratio
                    # spectum for the input time.
